<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>B</mml:mi></mml:math>-mode polarization of the CMB and the cosmic neutrino background

Mohammadi, Rohoollah; Khodagholizadeh, Jafar; Sadegh, Mahdi; Xue, She‐Sheng

doi:10.1103/physrevd.93.125029

Cited by 15 publications

(9 citation statements)

References 38 publications

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“…1. The fifth diagram in which two fermions directly couple to two photons is given in (21). Therefore, the amplitude of the Compton scattering in the NCQED can be given as…”

Section: Stokes Parameters and Boltzmann Equationmentioning

confidence: 99%

“…Furthermore, the Compton scattering in the presence of a background can potentially lead to a B-mode polarization for the CMB even for the scalar perturbation. The contribution to the observed B-mode spectrum from the interaction between CMB photon and the cosmic neutrino background (CNB) in the scalar perturbation background has been considered in [20,21].…”

Section: Introductionmentioning

confidence: 99%

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Cosmic microwave background polarization in non-commutative space-time

et al. 2016

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In the standard model of cosmology (SMC) the B-mode polarization of the CMB can be explained by the gravitational effects in the inflation epoch. However, this is not the only way to explain the B-mode polarization for the CMB. It can be shown that the Compton scattering in the presence of a background, besides generating a circularly polarized microwave, can lead to a B-mode polarization for the CMB. Here we consider the non-commutative (NC) spacetime as a background to explore the CMB polarization at the last scattering surface. We obtain the B-mode spectrum of the CMB radiation by scalar perturbation of metric via a correction on the Compton scattering in NC-space-time in terms of the circular polarization power spectrum and the non-commutative energy scale. It can be shown that even for the NC scale as large as 20 TeV the NC-effects on the CMB polarization and the r parameter are significant. We show that the V-mode power spectrum can be obtained in terms of linearly polarized power spectrum in the range of microto nano-kelvin squared for the NC scale of about 1-20 TeV, respectively.

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“…1. The fifth diagram in which two fermions directly couple to two photons is given in (21). Therefore, the amplitude of the Compton scattering in the NCQED can be given as…”

Section: Stokes Parameters and Boltzmann Equationmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Cosmic microwave background polarization in non-commutative space-time

et al. 2016

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“…Some of our recent works also discussed the generation of B-mode polarization in the presence of scalar perturbations via Cosmic Neutrino Background and CMB interactions [47,59,60], nonlinear photons interactions [61], photon interaction by considering extensions to QED such as Lorentzinvariant violating operators [62], non-commutative geometry [49], interaction of dipolar dark matter with CMB photons [63] and photon-fermion forward scattering [64]. Also the intrinsic B-mode polarization is calculated by using the Boltzmann code SONG [65] which induce in the CMB by the evolution of primordial density perturbations at second order [66].…”

Section: Introductionmentioning

confidence: 99%

B-mode power spectrum of CMB via polarized Compton scattering

Khodagholizadeh

Mohammadi

Sadegh

et al. 2020

J. Cosmol. Astropart. Phys.

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In this work, according to some evidence from being an asymmetry in the number density of left and right-handed electrons, δ L , in-universe motivate us to calculate the dominated contribution of this asymmetry in the generation of B-mode power spectrum C (S) B l . Note, in the standard cosmological scenario, Compton scattering in the presence of scalar matter perturbation can not generate magnetic like pattern in linear polarization while in the case of polarized Compton scattering, we have shown C (S) B l ∝ δ 2 L . We add up the spectrum of the B-mode generated by the polarized Compton scattering to the spectra produced by weak lensing effects and Compton scattering in the presence of tensor perturbations. The resultsshow a significant amplification in C B l in large scale l < 500 for δ L > 10 −6 which will be observable in future high resolution B-mode polarization detection. Finally, we have shown that C (S) B l generated by polarized Compton scattering can suppress the tensor to scalar ratio, r parameter so that this contamination can be comparable to a primordial tensor-to-scalar ratio spatially for δ L > 10 −5 . PACS numbers: 13.15.+g, 98.80.Es, 98.70.Vc. a j.gholizadeh@cgu.ac.ir b rmohammadi@ipm.ir c m.sadegh@pnu.ac.ir d vahedi@khu.ac.ir,vahedi@ipm.ir2

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“…As the new sources, for instance, in [36] the effect of the Faraday rotation due to the uniform magnetic field on the CMB is investigated and it is shown that a nonvanishing Bmode polarization can be produced through Faraday rotation. In [37,38], the authors have discussed that photon-neutrino interaction in the presence of scalar perturbations could be considered as one of the sources of the CMB B-mode polarization. It is also shown that the Compton scattering in the non-commutative space-time can generate the B-mode polarization of the CMB [39] and the possibility of the producing B-mode polarization pattern due to polarized Compton scattering in the presence of scalar perturbations has been discussed in [40].…”

Section: Introductionmentioning

confidence: 99%

Dipolar dark matter and CMB B-mode polarization

et al. 2020

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We consider dark matter particles as singlet fermionic particles carrying magnetic dipole moment to explore its contribution on the polarization of the cosmic microwave background (CMB) photons. We show that Dirac fermionic dark matter particles have no contribution on the CMB polarization. However, in the case of Majorana dark matter, this type of interaction leads to the B-mode polarization in the presence of primordial scalar perturbations which is in contrast with the standard scenario for the CMB polarization. We numerically calculate the B-mode power spectra and plot $$C_l^{BB}$$ClBB for different dark matter masses and the r-parameter. We show that dark matter particles with masses less than 100 MeV have a valuable contribution on $$C_l^{BB}$$ClBB. Meanwhile, dark matter particles with mass $$\text {m}_{\text {DM}}\le 50\, \text {MeV}$$mDM≤50MeV for $$r=0.07$$r=0.07 ( $$\text {m}_{\text {DM}}\le 80\, \text {MeV}$$mDM≤80MeV for $$r=0.09$$r=0.09) can be excluded experimentally. Furthermore, our results put a bound on the magnetic dipole moment about $$\text {M}\le 10^{-16} e\,\, \text {cm}$$M≤10-16ecm in agreement with the other reported constraints.

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B-mode polarization of the CMB and the cosmic neutrino background

Cited by 15 publications

References 38 publications

Cosmic microwave background polarization in non-commutative space-time

Cosmic microwave background polarization in non-commutative space-time

B-mode power spectrum of CMB via polarized Compton scattering

Dipolar dark matter and CMB B-mode polarization

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